bachelor's at Bacharelado em Física from Pontifícia Universidade Católica de São Paulo (1979), master's at Astronomy from Universidade de São Paulo (1982) and doctorate at Astronomy from Universidade de São Paulo (1989). He is currently professor associado at Universidade de São Paulo. Has experience in Astronomy, focusing on Stellar Astrophysics, acting on the following subjects: Alfvén waves, solar and stellar winds, Solar and astrophysical Alfvênic heating, solar activity, Sun-Earth interaction, heating of protostellar accretion disks. (Source: Lattes Curriculum)
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The theoretical study we have developed on the physical processes involved in star formation refer to winds of solar type stars and protostellar discs, seeking to better understand the formation and the early stages of evolution of these objects. In this project we intend to mount an observational picture of star formation to place links in the scenario currently accepted. For this we pro…
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The angular momentum transport in accretion disks associated to young stellar objects is a key mechanism in understanding and describing the evolution of stars -and planetary systems- in their early stages. Currently, there are two important mechanisms used to describe the angular momentum transport in accretion disks of T Tauri stars: the Magnetorotational Instability (MRI) and the magne…
T-Tauri stars in their more evolved stages have strong stellar winds and also surface magnetic fields around kG. Previous work has shown that the damping of Alfvén waves, created by turbulent movements at the base of the wind, can explain the observed speeds of these winds. The current and growing search for rocky exoplanets of dimensions comparable to Earth's makes it necessary a better …
The star formation region CMa R1 corresponds to a late stage star forming region, with past explosions of massive stars sustaining the star formation currently moderately active today, with a low fraction of circumstellar discs, and with a population of young "old" stars of low mass coexisting with much younger objects. Several studies, performed at different wavelengths in this region, h…
The plasma of the solar atmosphere loses energy by radiation and need a mechanical source of heat for maintaining the temperature in equilibrium. Many studies show that magneto-acoustic waves can balance the energy in some regions of the solar atmosphere. Specifically, these waves allow us to study the gas dynamic in structures as coronal loops and also to get the values of temperature, d…
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Focused on better understand the formation and early stages of evolution of young stars, especially those with active chromospheric activity, we propose, in continuation of the project that has been developed by Dr. Santos-Silva in her postdoctoral contract, an internship of 9 months at Eberhard Karls Universität Tübingen - Germany, in order to better learn the techniques used by Prof. Be…
Solar atmosphere plasma loses energy through radiation and thermal conduction and thus needs a mechanical heat source to maintain its temperature in equilibrium. In the literature, many theoretical and observational studies show us that magnetohydrodynamic waves can balance the energy in certain regions of the solar atmosphere. These waves allow us to study the gas dynamic in structures s…
| 31 / 23 | Completed research grants |
| 1 / 1 | Ongoing scholarships in Brazil |
| 16 / 5 | Completed scholarships in Brazil |
| 2 / 2 | Completed scholarships abroad |
| 50 / 31 | All research grants and scholarships |
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CV Lattes
ORCID